First and comprehensive study of V0757 Puppis: γ –Doradus pulsator in detached eclipsing binary

Pulsating stars in detached eclipsing binary systems are known for providing many important pieces of physical information which constrain both stellar structure and evolution theories. To date, fewer than 50 γ Doradus stars have been found in eclipsing binary systems, making them important targets in the study of g-mode pulsation inside the stars. We present a comprehensive physical and pulsational analysis of V0757 Puppis (TIC 6939791), a detached eclipsing binary system observed by the Transiting Exoplanet Survey Satellite mission (Sectors 7, 34, 61, and 88) and followed up with ground-based spectroscopy from the Thai National Telescope. By combining light curve modeling with radial velocities derived from medium-resolution spectra, we determined the fundamental stellar and atmospheric parameters with high precision. The system consists of an F2V primary (M₁=1.305± 0.026\, M_ , R₁=1.643± 0.020\, R_) and a G1V secondary (M₂=0.934± 0.030\, M_ , R₂=0.941± 0.079\, R_). We performed a detailed frequency analysis of the residual light curves, identifying two dominant independent pulsation frequencies at f~ 0.79\:c d⁻¹ and $0.98\:$c d⁻¹. These frequencies, along with the derived pulsation constant (Q~ 0.6\:d), confirm the primary component as a γ Doradus pulsator. An analysis of eclipse timing variations reveals non-detection of third-body companions with the currently available dataset, strengthened by the result of Gaia astrometric analysis. Evolutionary modeling indicates the system is ~2.2\:Gyr old, with the primary expected to fill its Roche lobe in ~1\:Gyr. Additionally, we calculate a distance of d≈ 350\:pc based on orbital and SED modeling, which is in excellent agreement with previous measurements using parallax distance.